In the past few years astronomical observations of neutron stars
[1]}, [2]}, [3]}, [4]}, [5]}, [6]}, [7]}, [8]}, [9]}, [10]}, [11]}, [12]}, [13]}, [14]}, [15]}, [16]}, [17]}, [18]}, [19]}, [20]}, [21]}, [22]}
have provided significant insight into the nuclear EoS at densities above \(n_{\rm sat}\) . This includes
quantities such as their mass, radius, and tidal deformability.
The EoS is given by the pressure, \(p\) , as a function of the energy density, \(e\) .
Analyses with piecewise polytropic EoS are useful [8]}, [9]}, [10]}, [11]}.
